1. L. Perivolaropoulos http://leandros.physics.uoi.gr Department of Physics University of Ioannina Open page

2. The consistency level of ΛCDM with geometrical data probes has been increasing with time during the last decade. There are some puzzling conflicts between ΛCDM predictions and specific observations (Dark Flow (velocity bulk flow), alignment and magnitude of low CMB multipoles, alignment of quasar optical polarization) Cosmological data for two new cosmological dipoles have emerged recently: Fine Structure Constant Dipole (4.1σ) Dark energy Dipole (2σ) From LP, 0811.4684 Webb et. al. Phys. Rev. Lett. 107, 191101 (2011) A. Mariano, L.P., arxiv:1206.4055, to appear in Phys. Rev. D.

3. Quasar absorption line spectra can determine the value of the fine structure constant at various redshifts and directions. The Keck+VLT sample consists of 295 absorbers with 0.2<z<4.2 and indicates a dipole angular distribution of the fine structure constant at 4.1σ confidence level. The distance moduli residuals from the ΛCDM best fit also exhibit a dipole anisotropy at the 2σ confidence level (0<z<1.4). This Dark Energy Dipole is obtained from the 557 SnIa of the Union2 sample. A. Mariano, L.P., arxiv:1206.4055, to appear in Phys. Rev. D. King et. al., arXiv:1202.4758 Webb et. al. Phys. Rev. Lett. 107, 191101 (2011)

4. Q1: What is the alignment level of these dipoles? Q2: What is the probability to produce the observed combination of these two dipoles in a homogeneous-isotropic cosmological model? Q3: What physical model has the potential to predict the existence of the above combined dipoles?

5. A1: The dark energy dipole and the α dipole are abnormally aligned with each other (angular separation 11.3 o ±11.8 o ) A2: The probability that the combined quasar absorber and SnIa data are obtained in the context of a homogeneous and isotropic cosmology is less than one part in 10 6. A3: There is a simple physical model based on a Hubble scale topological defect non-minimally coupled to electromagnetism that has the potential to explain the observed aligned dipoles. Q1: What is the alignment level of these dipoles? Q2: What is the probability to produce the observed combination of these two dipoles in a homogeneous-isotropic cosmological model? Q3: What physical model has the potential to predict the existence of the above combined dipoles?

6. Quasar Absorption Spectra: From absorption lines we can find both the absorber redshift and the value of the fine structure constant α=e 2 /hc at the time of absorption. Webb et. al. Phys. Rev. Lett. 107, 191101 (2011)

7. Quasar Absorption lines shift in different ways as we change α : x 10 -5 α =0.9 α 0 α=0.5 α 0 α = α 0 Absorption lines due to various atoms and ions x 10 -5 Flambaum et. al. Phys. Rev. Lett. 82, 888 (1999)] Webb et al. [Phys. Rev. Lett. 87, 091301 (2001) Northern hemisphere data Keck Tescope in Hawaii Many Multiplet Method: Use several absorption lines (iron and magnesium) simultaneously to determine α

8. Keck Telescopes in Hawaii (North)VLT in Chile (South) Other study of Many Multiplet Method (VLT): Webb et. al. Phys. Rev. Lett. 107, 191101 (2011) King et. al., MNRAS,422, 3370, (2012) (23 absorbers, underestimated errors) 295 absorbers

9. Oklo natural reactor bounds From T. Chiba, arxiv: 1111.0092

10. King et. al., MNRAS,422, 3370, (2012) Dipole+Monopole Maximum Likelihood Fit: 295 absorbers 4 parameters l= 320 o, b=-11 o

11. Random number from Gaussian probability distribution 10 4 Isotropic Monte Carlo Keck+VLT samples: None had as large a dipole magnitude as the observed!

12. http://leandros.physics.uoi.gr/defsdipoles/ Distance modulus: Luminosity Distance (flat): Emulate dipole+monopole fit of α: 557 SnIa standard candles

13. brighter SnIa smaller μ l= 309 o, b=-15 o

14. Random number from Gaussian probability distribution 10 4 Isotropic Monte Carlo Union2 samples: 4.75% had as large or larger a dipole magnitude A as the observed!

15. Random number from Gaussian probability distribution 10 4 Isotropic Monte Carlo Union2 samples: 6.12% had as small or smaller angular separation of dipole with fine structure dipole!

17. Angular separation of fine structure dipoles with full dark energy dipole in various redshift bins Angular separation of dark energy dipoles with full fine structure dipole in various redshift bins

18. What is the probability to obtain as large (or larger) dipole magnitudes with the observed alignment in an isotropic cosmological model? The fraction of isotropic Monte Carlo Keck+VLT datasets that can reproduce the obverved dipole magnitude is less than 0.01% The fraction of isotropic Monte Carlo Union2 datasets that can reproduce the obverved dipole magnitude and the observed alignment with Keck+VLT dipole is less than 1% 0.01% x 1% = 0.0001%

19. Is there a physical model that predicts the existence of such aligned dipoles? A. Mariano, L.P., Phys. Rev. D (to appear) arxiv:1206.4055 J. B. Sanchez, LP, Phys.Rev. D84 (2011) 123516 arxix:1110.2587 J. Grande, L.P., Phys. Rev. D 84, 023514 (2011).

20. Global Monopole Configuration: Non-minimally coupled scalar field Fine Structure Constant: Fine Structure Constant Spatial Variation:

21. Global Monopole: Field Direction in Space and Energy Density Off-center Observer

22. Lagrangian Density: Field Equations: Special Case: Non-minimally coupled Vortex: Field ansatz: Coaxial Magnetic Field Vortex

23. Field equations: Energy Density: Possible instability due to negative kinetic term

24. Correlation between value of fine structure constant and strong external magnetic fields. Peculiar velocity field (Dark Flow) in direction of lower acceleration Dark Flow Direction: (l,b)= (287 o ± 9 o,8 o ± 6 o ) Watkins et. al. arxiv: 0809.4041, Kashlinsky et. al. arxiv: 0809.3734

25. Maximum Temperature Difference Between Opposite Pixels along the Dipole Axes Large CMB temperature difference on opposite regions in the sky Mean Temperature Difference should be largest along the dipole directions (ISW CMB perturbations due to Global Monopole) WMAP 7yrs ILC map.

26. Maximum Temperature Difference (opposite pixels) ΔΤ=0.15mK Temperature Difference Map: Each pixel is replaced by its temperature difference with the opposite pixel (pixel scale 15 o ) Opposite Regions in the CMB Sky (l,b)= (157 o ± 15 o,+10 o ± 15 o ) ---(l,b)= (337 o ± 15 o,-10 o ± 15 o ). Healpix Pixelization (Nside=4) 180 o 360 o

27. Dark Flow Direction Watkins et. al. arxiv: 0809.4041, Kashlinsky et. al. arxiv: 0809.3734 WMAP7 ILC Map – Maximum Temperature Difference 15 o Pixel Pair (A. Mariano, LP in progress) Dark Energy Dipoleα Dipole Q1: How anomalous is this coincidence? A: Work in progress Q2: What are the detailed predictions of Extended Topological Quintessence

28. Early hints for deviation from the cosmological principle and statistical isotropy are being accumulated. This appears to be one of the most likely directions which may lead to new fundamental physics in the coming years. A simple mechanism that has the potential to give rise to such an alignment of Cosmological Axes is based on an off-center observer in a spherical energy inhomogeneity induced by a non-minimally coupled to electromagnetism, topologically non-trivial scalar field (Extended Topological Quintessence) Four Cosmologically Observed axes appear to be abnormally mutually aligned: The Fine Structure Constant Dipole (4σ) The Dark Energy Dipole (2σ) The Dark Flow Axis (3σ) The CMB Maximum Temperature Difference Axis (1.5 σ)